PSFEx extracts models of the PSF from FITS images processed with SExtractor, and measures the quality of images. The generated PSF models can be used for model-fitting photometry or morphological analyses.

Python package for making visuals of gravitational wave signals, specifically pulsar timing array signals.

This package provides tools for machine learning and data mining in astronomy.

This package contains a helper functionality to test ROMAN and JWST.

This package contains FIT and CSV files required for WebbPSF installation and distributed separately from it.

CFITSIO provides simple high-level routines for reading and writing Flexible Image Transport System files that insulate the programmer from the internal complexities of the FITS format. CFITSIO also provides many advanced features for manipulating and filtering the information in FITS files.

This package provides a range of colormaps designed for scientific use with Matplotlib. It includes perceptually uniform sequential colormaps such as abre, dusk, kepl, and octarine, as well as monochromatic sequential colormaps like blue, green, and red, and others (algae, pastel, and xray).

The FITS "World Coordinate System" (WCS) standard defines keywords and usage that provide for the description of astronomical coordinate systems in a FITS (Flexible Image Transport System) image header.

PyVO is a package providing access to remote data and services of the Virtual observatory (VO) using Python.

This package provides a Python module to various STScI image array manipulation functions.

pyHalo renders full mass distributions for substructure lensing simulations with gravitational lensing software package lenstronomy. The main purpose of the code is to quickly render full populations of dark matter subhalos and line of sight halos for gravitational lensing simulations. It also transltes halo properties (mass, concentration, redshift, etc) into angular units for lensing computations with lenstronomy.

This package implement functionality for computation of non-thermal radiation from relativistic particle populations. It includes tools to perform MCMC fitting of radiative models to X-ray, GeV, and TeV spectra using emcee, an affine-invariant ensemble sampler for Markov Chain Monte Carlo.

CZML3 is a Python library to write CZML, a JSON format for describing a time-dynamic graphical scene, primarily for display in a web browser running Cesium.

CAMB is a cosmology code for calculating cosmological observables, including CMB, lensing, source count and 21cm angular power spectra, matter power spectra, transfer functions and background evolution. The code is in Python, with numerical code implemented in fast modern Fortran.

This package provides a CLI and Python module to quickly calculate cosmological parameters e.g. redshift or luminosity-distance.

This package provides a CIANNA - a general-purpose deep learning framework primarily developed and used for astronomical data analysis.

TANGOS is a tool to build a database (along the lines of Eagle or MultiDark) for cosmological and zoom simulations.

Features:

• designed to store and manage results from custom analysis code

• provides web and Python interfaces

• science-focussed queries across entire merger trees, without requiring any knowledge of SQL

• manages the process of populating the database with science data, including auto-parallelising custom analysis

• customization with multiple Python modules such as pynbody or yt to process raw simulation data

• suports file-based database SQLite, server-based MySQL and PostgreSQL

ndcube is a package for manipulating, inspecting and visualizing multi-dimensional contiguous and non-contiguous coordinate-aware data arrays.

It combines data, uncertainties, units, metadata, masking, and coordinate transformations into classes with unified slicing and generic coordinate transformations and plotting/animation capabilities. It is designed to handle data of any number of dimensions and axis types (e.g. spatial, temporal, spectral, etc.) whose relationship between the array elements and the real world can be described by WCS translations.

CalcMySky is a software package that simulates scattering of light by the atmosphere to render daytime and twilight skies (without stars). Its primary purpose is to enable realistic view of the sky in applications such as planetaria. Secondary objective is to make it possible to explore atmospheric effects such as glories, fogbows etc., as well as simulate unusual environments such as on Mars or an exoplanet orbiting a star with a non-solar spectrum of radiation.

This package consists of three parts:

• calcmysky utility that does the precomputation of the atmosphere model to enable rendering.

• libShowMySky library that lets the applications render the atmosphere model.

• ShowMySky preview GUI that makes it possible to preview the rendering of the atmosphere model and examine its properties.

Astropy is a single core package for Astronomy in Python. It contains much of the core functionality and some common tools needed for performing astronomy and astrophysics.

astrodata is a package for managing astronomical data through a uniform interface. It is designed to be used with the Astropy package. astrodata was created for use as part of the DRAGONS data reduction pipeline, but it is now implemented to be useful for any astronomical data reduction or analysis project.

Unlike managing files using the astropy.io.fits package alone, astrodata is designed to be extendible to any data format, and to parse, respond to, and store metadata in a consistent, intentional way. This makes it especially useful for managing data from multiple instruments, telescopes, and data generation utilities.

This package includes a plugin for the Python library ASDF to add support for reading and writing various compression algorithms including: Blosc,LZ4 Frame,Zstandard.

Tempo analyzes pulsar timing data. Pulse times of arrival (TOAs), pulsar model parameters, and coded instructions are read from one or more input files. The TOAs are fitted by a pulse timing model incorporating transformation to the solar-system barycenter, pulsar rotation and spin-down and, where necessary, one of several binary models. Program output includes parameter values and uncertainties, residual pulse arrival times, chi-squared statistics, and the covariance matrix of the model. In prediction mode,ephemerides of pulse phase behavior (in the form of polynomial expansions) are calculated from input timing models.

This package provides a structured, variable-resolution meshes, unstructured meshes, and discrete or sampled data such as particles. Focused on driving physically-meaningful inquiry, it has been applied in domains such as astrophysics, seismology, nuclear engineering, molecular dynamics, and oceanography.